The Presupernova Core Mass–Radius Relation of Massive Stars: Understanding Its Formation and Evolution
The Presupernova Core Mass–Radius Relation of Massive Stars: Understanding Its Formation and Evolution
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大质量恒星的前超新星核心质量-半径关系：了解其形成和演化
DOI：
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发表时间：
2019
影响因子：
4.9
通讯作者：
M. Limongi
中科院分区：
文献类型：
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作者：
A. Chieffi;M. Limongi
我们提供了一个从主序星到坍缩开始的大质量恒星（12 ≤ M（）≤ 27.95范围内的320颗）的太阳金属丰度模型的精细网格，以定量地确定它们的致密性（奥康纳和Ott定义的致密性2.5）如何与核心坍缩开始时的碳氧核心质量成比例。我们发现了一个明确的，非单调（但不是分散）的趋势与碳-氧核心质量的紧密性是严格（主要）相关的行为，即，在进化的高级阶段，各种碳对流事件的诞生、发展和消失。虽然碳氧核心的质量大小和中心氦燃烧后留下的12 C的数量在塑造最终的质量-半径关系中起着重要作用，但最终决定星星最终致密程度的是12 C的丰度，因为它控制着碳燃烧壳层在最终坍缩前质量增长的能力。
We present a fine grid of solar metallicity models of massive stars (320 in the range 12 ≤ M( ) ≤ 27.95), extending from the main sequence up to the onset of the collapse, in order to quantitatively determine how their compactness ξ2.5, defined by O’Connor & Ott, scales with the carbon–oxygen core mass at the beginning of core collapse. We find a well defined, nonmonotonic (but not scattered) trend of the compactness with the carbon–oxygen core mass that is strictly (and mainly) correlated to the behavior, i.e., birth, growth, and disappearance, of the various carbon convective episodes that follow one another during the advanced evolutionary phases. Though both the mass size of the carbon–oxygen core and the amount of 12C left by the central He burning play a major role in sculpting the final mass–radius relation, it is the abundance of 12C that is ultimately responsible for the final degree of compactness of a star, because it controls the ability of the carbon-burning shell to advance in mass before the final collapse.
9、10、11、12 和 13 M 星的三维超新星爆炸模拟
影响因子：
4.8
作者：
Burrows, Adam;Radice, David;Vartanyan, David
通讯作者：
Vartanyan, David